  The discovery of young globular clusters in merging galaxies and other
environments provides an opportunity to study directly the process of globular
cluster formation. Empirically it appears that globular cluster formation
occurs preferentially in regions in which star formation occurs at a high rate
and efficiency. Further, the interstellar medium in such regions is likely to
be at a higher pressure than less active star-forming environments. An
additional observational clue to the globular cluster formation process is that
young globular clusters have little or no mass-radius relationship. In this
paper I argue that high pressure and high star-formation efficiency are
responsible for current globular cluster formation. I suggest that the
precursors to globular clusters are molecular clouds and that the mass-radius
relationship exhibited by such clouds is wiped out by a variable star formation
efficiency.
