  Curvature perturbations generated after the end of inflation are estimated
for a generic multi-field inflationary potential. The curvature perturbations
are generated by conversion of inflationary isocurvature perturbations, similar
to curvaton and inhomogeneous reheating scenarios. During inflation, the
trajectory along which the fields are rolling down will fluctuate. When
inflation ends, the fields enter the oscillatory phase along different
directions in different parts of the universe. Different oscillatory
trajectories can have different effective equations of state and reheating
rates, so that different parts of the universe will evolve differently. This
translates the isocurvature perturbations into the curvature perturbations.
  If all light fields make similar contributions to the potential energy, the
postinflationary curvature perturbations are much smaller than the standard
inflationary curvature perturbations. But if different light fields make very
different contributions to the potential energy, the postinflationary curvature
perturbations can exceed the inflationary perturbations. The characteristic
feature of postinflationary perturbations is non-Gaussianity $\sim \pm 1$.
