  Some factors connecting the evolutionary histories of galaxies with the
characteristics of their cluster systems are reviewed. Unanswered questions
include: How is one to understand the observation that some globular cluster
systems have disk kinematics whereas others do not? Why do some galaxies have
cluster systems with unimodal metallicity distributions, whereas others have
bimodal metallicity distributions? What caused the average ellipticity of
individual clusters to differ from galaxy to galaxy?
