  We present evidence that clumps of \lya lines are physically associated with
about half of the extensive metal-line systems (absorption systems with four or
more observed metal-line species) found in this paper, demonstrate that all
four \lylimit systems discussed here correspond to extensive metal-line
absorption systems, and present an extraordinary pair of extensive metal-line
absorption systems within 2000~km/s of each other at $z~=~0.95$ that are
probably an early manifestation of large scale structure. These results are
obtained using ultraviolet spectra, taken with the higher-resolution gratings
of the Faint Object Spectrograph of the Hubble Space Telescope, for four
quasars with emission-line redshifts between 1.0 and 1.3. We also determine the
evolution of \lya absorption lines at redshifts less than 1.3 by combining the
results for 13 smaller redshift quasars discussed in Paper I of this series
with the 4 moderate redshift quasars analyzed in the present paper. For $z_{\rm
abs}~\leq~1.3$, the density of \lya lines with equivalent widths greater than
0.24~\AA\ is adequately fit by $\left(dN/dz\right) =\left(dN/dz\right)_0
\cdot(1 + z)^\gamma$ with $(dN/dz)_0 = 24.3 \pm 6.6$ \lya lines per unit
redshift, and $\gamma = 0.58 \pm 0.50$ (1-$\sigma$ uncertainties). This rate of
evolution at low redshifts is less than the evolutionary rate inferred from
several different ground-based data samples that pertain to high redshifts. The
observed gaseous structures at redshifts of $0.5$ to $1.0$ with velocity
dispersions of $6 \times 10^2$ \kms to $1.4 \times 10^3$ \kms (or velocity
spans of $1.2 \times 10^3$ \kms to $3 \times 10^3$ \kms) constitute a
constraint on cosmological models of structure formation.
