  When applied to deep photometric catalogs, the two-point angular correlation
function, w(theta), is a sensitive probe of the evolution of galaxy clustering
properties. Here we present measurements of w(theta) as a function of I_AB
magnitude and (R-I) color to a depth of I_AB=24, using a sample of ~350,000
galaxies covering 5 degrees^2 in total over 5 separate fields. Using redshifts
of 3319 galaxies in early DEEP2 Galaxy Redshift Survey data, we construct
robust galaxy redshift distributions as a function of I_AB and R_AB magnitude
and (R-I) color for galaxies between 0<z<2. We constrain models of the redshift
evolution of galaxy clustering and find that significant growth of clustering
has occurred from z>1 to z=0. A model in which the comoving scale-length, x_0,
evolves linearly with redshift, x_0(z)=x_0(0)(1-Bz), fits the data better than
the 'epsilon' model proposed by Groth and Peebles (1977). The clustering
properties depend strongly on observed (R-I) color, with both the reddest and
bluest galaxies exhibiting large clustering amplitudes and steeper slopes.
Different observed (R-I) color ranges are sensitive to very disparate redshift
regimes. Red galaxies with (R-I)~1.5 lie in a narrow redshift range centered at
z~0.85 and have a comoving scale length of clustering at z=0.85 of x_0=5.0
+/-0.3 Mpc/h. These galaxies have early-type spectra and are likely progenitors
of massive local ellipticals. The bluest galaxies with (R-I)~0 appear to be a
mix of star-forming galaxies, both relatively local (z~0.3-0.6) dwarfs and
bright z>1.4 galaxies, and broad-line AGN. We find that local blue dwarfs are
relatively unclustered, with x_0=1.6 +/-0.2 Mpc/h. The z>1.4 blue galaxies have
a larger clustering scale-length, x_0>5 Mpc/h.
