  The ensemble of now more than 250 discovered planetary systems displays a
wide range of masses, orbits and, in multiple systems, dynamical interactions.
These represent the end point of a complex sequence of events, wherein an
entire protostellar disk converts itself into a small number of planetary
bodies. Here, we present self-consistent numerical simulations of this process,
which produce results in agreement with some of the key trends observed in the
properties of the exoplanets. Analogs to our own solar system do not appear to
be common, originating from disks near the boundary between barren and (giant)
planet-forming.
