  We study the dynamical evolution of disk and halo globular clusters in the
Milky Way using a series of Fokker-Planck calculations combined with parametric
statistical models. Our sample of 113 clusters with velocity data is predicted
to descend from an initial population of 250 clusters, implying more than a
factor of two decrease in population size due to evolution.
  Approximately 200 of these clusters are in a halo component and 50 in a disk
component. The estimated initial halo population follows a coreless R^{-3.38}
density profile in good agreement with current estimates for the distribution
of halo field stars. The observed core in the present-day distribution of halo
clusters results from the rapid evaporation of clusters in the inner regions of
the Galaxy. The initial halo population is also predicted to have a radially
biased orbit distribution in rough agreement with the observed kinematics of
halo field stars. The isotropy of the present-day halo cluster distribution
results from the evaporation of clusters on elongated orbits. Similarly, the
initial disk component has a nearly isotropic initial distribution that becomes
more tangentially biased with time. However, the inferred initial
characteristics of the disk component do not match the kinematics of the
rapidly rotating thin or thick disk stellar populations. These characteristics
may be more indicative of the flattened halo component discussed by Zinn
(1993).
  Detailed examination of cluster evolution confirms the importance of disk
heating. Clusters on low-inclination orbits experience the strongest disk
heating because of optimal matches in resonant frequencies. Disk heating on
high-inclination orbits is weaker but still dominates over spheroidal heating.
