  We combine new and archival Chandra observations of the globular cluster NGC
6752 to create a deeper X-ray source list, and study the faint radio
millisecond pulsars (MSPs) of this cluster. We detect four of the five MSPs in
NGC 6752, and present evidence for emission from the fifth. The X-rays from
these MSPs are consistent with thermal emission from the neutron star surfaces,
with significantly higher fitted blackbody temperatures than other globular
cluster MSPs (though we cannot rule out contamination by nonthermal emission or
other X-ray sources). NGC 6752 E is one of the lowest-L_X MSPs known, with
L_X(0.3-8 keV)=1.0+0.9-0.5*10^30 ergs/s. We check for optical counterparts of
the three isolated MSPs in the core using new HST ACS images, finding no
plausible counterparts, which is consistent with their lack of binary
companions. We compile measurements of L_X and spindown power for radio MSPs
from the literature, including errors where feasible. We find no evidence that
isolated MSPs have lower L_X than MSPs in binary systems, omitting binary MSPs
showing emission from intrabinary wind shocks. We find weak evidence for an
inverse correlation between the estimated temperature of the MSP X-rays and the
known MSP spin period, consistent with the predicted shrinking of the MSP polar
cap size with increasing spin period.
