  The two-point angular correlation function of galaxies, \wte, has been
computed from a new survey of faint galaxies covering a 2 deg$^2$ area near the
North Galactic Pole. This survey, which is complete to limiting magnitudes
\jmag=24 and \fmag=23, samples angular scales as large as $1\degpoint5$. Faint
galaxies are found to be more weakly clustered (by a factor of at least two)
compared to galaxies observed locally. Clustering amplitudes are closer to
model predictions in the red than in the blue. The weak clustering of faint
galaxies cannot be explained by any plausible model of clustering evolution
with redshift. However, one possible explanation of the clustering properties
of intermediate redshift galaxies is that they resemble those of starburst
galaxies and H II region galaxies, which are observed locally to possess weak
clustering amplitudes. Our clustering amplitudes are also similar to those of
nearby late-type galaxies, which are observed to be more weakly clustered than
early-type galaxies A simple, self-consistent model is presented that predicts
the fraction of galaxies in the ``excess'' population at intermediate
redshifts, and correctly matches observed color distributions. The available
data on the clustering properties of faint galaxies are consistent with this
model if the ``excess'' population of faint blue galaxies is also the weakly
clustered population. Evidence is presented that the power-law slope of the
angular correlation function becomes shallower at fainter magnitudes. A similar
effect is seen locally both for dwarf galaxies and for galaxies with late
morphological type;
