  We describe comprehensive calculations of the formation of icy planets and
debris disks at 30-150 AU around 1-3 solar mass stars. Disks composed of large,
strong planetesimals produce more massive planets than disks composed of small,
weak planetesimals. The maximum radius of icy planets ranges from roughly 1500
km to 11,500 km. The formation rate of 1000 km objects - `Plutos' - is a useful
proxy for the efficiency of icy planet formation. Plutos form more efficiently
in massive disks, in disks with small planetesimals, and in disks with a range
of planetesimal sizes. Although Plutos form throughout massive disks, Pluto
production is usually concentrated in the inner disk. Despite the large number
of Plutos produced in many calculations, icy planet formation is inefficient.
At the end of the main sequence lifetime of the central star, Plutos contain
less than 10% of the initial mass in solid material. This conclusion is
independent of the initial mass in the disk or the properties of planetesimals.
Debris disk formation coincides with the formation of planetary systems
containing Plutos. As Plutos form, they stir leftover planetesimals to large
velocities. A cascade of collisions then grinds the leftovers to dust, forming
an observable debris disk. In disks with small (< 1-10 km) planetesimals,
collisional cascades produce luminous debris disks with maximum luminosity
roughly 0.01 times the stellar luminosity. Disks with larger planetesimals
produce much less luminous debris disks. Observations of debris disks around
A-type and G-type stars strongly favor models with small planetesimals. In
these models, our predictions for the time evolution and detection frequency of
debris disks agree with published observations. We suggest several critical
observations that can test key features of our calculations.
