  We present results for the two-point angular correlation function of galaxies
to a limiting magnitude of r=26. The final sample is 97% complete to r=26.0,
yielding 5730 galaxies over a 90.1 sq. arcmin field. The correlation function
for our faint galaxies can be parameterised by a power law, $A \theta^{-0.8}$,
in agreement with the clustering statistics of shallower catalogues. The
derived amplitude, $A$, is small, but non-zero. We combine this measurement
with the latest statistical constraints on faint galaxy redshifts from
gravitational lensing studies, which imply that the bulk of the r<26 field
galaxies should be at redshifts of order 1. Our derived $A$ is significantly
lower than that predicted from the local bright galaxy correlation function
using the lensing-determined galaxy redshift distribution and modest growth of
clustering. This simplistic model does not include the variation in observed
morphological mix as a function of redshift and apparent magnitude in our
sample. At our faintest limits we reach sufficiently high redshifts that
differential $K$ corrections will result in the observed galaxy mix being
dominated by star bursting dwarf and low surface brightness irregulars, rather
than the early-type systems used to define the local bright galaxy correlation
function. Adopting the correlation function measured locally for these low
surface brightness galaxies and assuming modest clustering evolution, we obtain
reasonable agreement between our model and observations. This model supports
the scenario in which the high number density of faint galaxies is produced by
normally clustered star forming dwarf galaxies at modest redshifts.
