  A clustering analysis is performed on two samples of $\sim 600$ faint
galaxies each, in two widely separated regions of the sky, including the Hubble
Deep Field. One of the survey regions is configured so that some galaxy pairs
span angular separations of up to 1 deg. The median redshift is $z_{med}\approx
0.55$. Strong clustering is obvious, with every pencil-beam field containing a
handful of narrow redshift-space features, corresponding to galaxy structures
with sizes of 5 to 20 Mpc. The structures are not obviously organized on
planes, though one prominent, colinear triplet of structures is observed,
spanning $\sim 20$ Mpc. This may be evidence of a filament. A galaxy--galaxy
correlation function calculation is performed. No significant evolution of
clustering (relative to stable clustering) is found in the redshift range
0.3<z<1.0. This is not surprising, since uncertainties in the correlation
amplitude estimated from surveys like these are large; field-to-field
variations and covariances between data points are both shown to be
significant. Consistent with other studies in this redshift range, the
galaxy--galaxy correlation length is found to be somewhat smaller than that
predicted from local measurements and an assumption of no evolution. Galaxies
with absorption-line-dominated spectra show much stronger clustering at
distances of <2 Mpc than typical field galaxies. There is some evidence for
weaker clustering at intermediate redshift than at low redshift, when the
results presented here are compared with surveys of the local Universe. In
subsets of the data, the measured pairwise velocity dispersion of galaxies
ranges from 200 to $600 km s^{-1}$, depending on the properties of the dominant
redshift structures in each subset.
