  We analyzed the spatial distribution of 28500 photometrically selected
galaxies with AB magnitude 23.5<R<25.5 and redshift 1.4<z<3.5 in 21 fields with
a total area of 0.81 square degrees. The galaxies were divided into three
subsamples, with mean redshifts z=1.7, 2.2, 2.9, according to the UGR selection
criteria of Adelberger et al. (2004) and Steidel et al. (2003). Combining the
galaxies' measured angular clustering with redshift distributions inferred from
1600 spectroscopic redshifts, we find comoving correlation lengths at the three
redshifts of r_0 = 4.5+-0.6, 4.2+-0.5, and 4.0+-0.6 h^-1 Mpc, respectively, and
infer a roughly constant correlation function slope of gamma=1.6+-0.1. We
derive similar numbers from the 1600 object spectroscopic sample itself with a
new statistic, K, that is insensitive to many possible systematics. Galaxies
that are bright in R (lambda_rest ~ 1500-2500A) cluster more strongly than
fainter galaxies at z=2.9 and z=2.2 but not, apparently, at z=1.7. Comparison
to a numerical simulation that is consistent with recent WMAP observations
suggests that galaxies in our samples are associated with dark matter halos of
mass ~ 10^12, and that a small fraction of the halos contain more than one
galaxy that satisfies our selection criteria. Adding recent observations of
galaxy clustering at z~0 and z~1 to the simulation results, we conclude that
the typical object in our samples will evolve into an elliptical galaxy by
redshift z=0 and will already have an early-type spectrum by redshift z=1. We
comment briefly on the implied relationship between galaxies in our survey and
those selected with other techniques. (slightly abridged)
