We discuss the origin of physical properties of globular cluster
systems (GCSs) in galaxies in terms of galaxy formation and evolution
processes. Based on numerical simulations of dynamical evolution
of GCSs in galaxies, we particularly discuss (1) the origin of
radial density profiles of GCSs, (2) kinematics of GCSs in elliptical
galaxies, (3) transformation from nucleated dwarf galaxies into GCs 
(e.g., omega Centauri), (4) the origin of GCSs in the Large Magellanic
Cloud,  and (5) formation of intragroup and intracluster GCs.