  Quiescent low-mass X-ray binaries (qLMXBs) containing neutron stars have been
identified in several globular clusters using Chandra or XMM X-ray
observations, using their soft thermal spectra. We report a complete census of
the qLMXB population in these clusters, identifying three additional probable
qLMXBs in NGC 6440. We conduct several analyses of the qLMXB population, and
compare it with the harder, primarily CV, population of low-luminosity X-ray
sources with 10^31<L_X<10^32.5 ergs/s. The radial distribution of our qLMXB
sample suggests an average system mass of 1.5^{+0.3}_{-0.2} Msun, consistent
with a neutron star and low-mass companion. Spectral analysis reveals that no
globular cluster qLMXBs, other than the transient in NGC 6440, require an
additional hard power-law component as often observed in field qLMXBs. We
identify an empirical lower luminosity limit of 10^32 ergs/s among globular
cluster qLMXBs. The bolometric luminosity range of qLMXBs implies (in the deep
crustal heating model of Brown and collaborators) low time-averaged mass
transfer rates, below the disk stability criterion. The X-ray luminosity
functions of the CV populations alone in NGC 6397 and 47 Tuc are shown to
differ. The distribution of qLMXBs among globular clusters is consistent with
their dynamical formation by either tidal capture or exchange encounters,
allowing us to estimate that seven times more qLMXBs than bright LMXBs reside
in globular clusters. The distribution of harder sources (primarily CVs) has a
weaker dependence upon density than that of the qLMXBs. Finally, we discuss
possible effects of core collapse and globular cluster destruction upon X-ray
source populations.
