We propose a self-consistent model for globular cluster formation in,
but not limited to, our Galaxy, based on the merger model of Mathews &
Schramm (1993). Stars and star clusters form in bursts at the merging
interfaces as protogalactic clouds collide. We describe the formation
of those star clusters with a simple schematic Ansatz which takes int
o account the thermal and Kelvin-Helmholtz instabilities. It is shown
that this model is consistent with many observational properties such
as the age and metallicity distributions of globular clusters, the ove
rall number of globular clusters, and the near constancy of the number
s of globular clusters in different size host galaxies. Most of the fe
atures of this merger model are insensitive to choices of parameters.
However, the model does not produce as many high-metallicity clusters
as observed. Possible explanations for this are presented.