  We investigate the dynamics of inflation models driven by multiple, decoupled
scalar fields and calculate the Hubble parameter and the amplitude of the
lightest field at the end of inflation which may be responsible for
interesting, or possibly dangerous cosmological consequences after inflation.
The results are very simple and similar to those of the single field inflation,
mainly depend on the underlying spectrum of the masses. The mass distribution
is heavily constrained by the power spectrum of density perturbations P and the
spectral index n. The overall mass scale gives the amplitude of P, and n is
affected by the number of fields and the spacing between masses in the
distribution. The drop-out effect of the massive fields makes the perturbation
spectrum typically redder than the single field inflation spectrum. We
illustrate this using two different mass distributions.
