In the self-production regime new regions of $_{H}$− 1 inf prop up on a timescale of one e- folding with field values ∼ φ ± Δ φ/ 2, where Δ φ ∼ H$_{inf}$/ 2 π . In such regions quantum fluctuations dominate over the classical slow-roll of the field. After few e-foldings, N , these regions are locally homogeneous and grow almost independently. The correla- tion between the two regions 〈 φ + Δ φ/ 2 , φ − Δ φ/ 2 〉 ∼ e − $^{N}$, die exponentially. Such self-reproduction regions in the inflationary potential can solve the initial homogeneity problem without any trouble. This is also known as eternal inflation $^{21}$. Also note that chaotic initial conditions can be obtained for low scale models of infla- tion provided the potential is extremely flat. For instance, near the saddle point φ$_{0}$ of a potential, V ′ ( φ$_{0}$ ) = 0 , V ′′ ( φ$_{0}$ ) = 0, the quantum fluctuations will dominate over classical motion in a range Δ φ ≪ M$_{P}$ . Such regions will support self-reproduction of space-time with locally homogeneous regions. However as we shall argue that in order to reach a plateau of such a low scale inflationary potential one requires stochastic jumps of the inflaton field during a prior phase of inflation [90, 284]. Furthermore, if inflation is driven by a collection of scalar fields as in the case of assisted inflation , then the initial condition problem for a single field chaotic inflation model can be ameliorated, as one would not require super-Planckian VEVs for the inflatons [285–287]. 21 Note that inflation is not past eternal. The first argument is based on singularity theorems due to Hawking-Penrose [143]. The large stochastic fluctuations cannot take the field forever up the potential. When the field fluctuations become non-linear in one Hubble region, the entire region would collapse to form a blackhole. The second reason is due to [144], where it has been argued that null and time like geodesics are past-incomplete during inflation as long as the averaged expansion rate is such that H$_{av}$ > 0 holds along the past directed geodesics. The observers along these geodesics would take finite amount of time to hit the singularity. • Problems with a large VEV: A natural question arises for many models: can we trust the effective field theory treatment of an inflaton potential when the VEV of the field is super-Planckian. The answer is no, in particular when the inflaton has couplings to the SM or MSSM degrees of freedom. An effective field theory treatment is trustable only when the momentum is bounded by the cut-off as well as the total energy density is below the Planckian energy density. For any renormalizable coupling between the inflaton and any matter 34