We present a catalog of 422 galaxies with published measurements of their globular cluster (GC) populations. Of these, 248 are E galaxies, 93 are SO galaxies, and 81 are spirals or irregulars. We also present updated versions of the GC specific frequency S sub(N) and specific mass S sub(M) versus host galaxy luminosity and baryonic mass. These graphs exhibit the previously known U-shape: highest S sub(N) or S sub(M) values occur for either dwarfs or supergiants, but in the midrange of galaxy size (10 super(9)-10 super(10) L sub(middot in circle)) the GC numbers fall along a well-defined baseline value of S sub(N) Asymptotically = to 1 or S sub(M) = 0.1, similar among all galaxy types. Our results strongly reinforce recent proposals that GC formation efficiency appears to be most nearly proportional to the galaxy halo mass M sub(halo). Finally, we find that an excellent empirical predictor of total GC population for galaxies of all luminosities is N sub(GC) ~ (R sub(e)sigma sub(e)) super(1.3), a result consistent with fundamental plane scaling relations.