  We present a statistical study of the post-formation migration of giant
planets in a range of initial disk conditions. For given initial conditions we
model the evolution of giant planet orbits under the influence of disk,
stellar, and mass loss torques. We determine the mass and semi-major axis
distribution of surviving planets after disk dissipation, for various disk
masses, lifetimes, viscosities, and initial planet masses. The majority of
planets migrate too fast and are destroyed via mass transfer onto the central
star. Most surviving planets have relatively large orbital semi-major axes of
several AU or larger. We conclude that the extrasolar planets observed to date,
particularly those with small semi-major axes, represent only a small fraction
(~25% to 33%) of a larger cohort of giant planets around solar-type stars, and
many undetected giant planets must exist at large (>1-2 AU) distances from
their parent stars. As sensitivity and completion of the observed sample
increases with time, this distant majority population of giant planets should
be revealed. We find that the current distribution of extrasolar giant planet
masses implies that high mass (more than 1-2 Jupiter masses) giant planet
formation must be relatively rare. Finally, our simulations imply that the
efficiency of giant planet formation must be high: at least 10% and perhaps as
many as 80% of solar-type stars possess giant planets during their pre-main
sequence phase. These predictions, including those for pre-main sequence stars,
are testable with the next generation of ground- and space-based planet
detection techniques
