  Terzan 5 is a rich globular cluster within the galactic bulge that contains
39 known millisecond pulsars, the largest known population of any globular
cluster. The Terzan 5 pulsars are faint, so that individual observations of
most of the pulsars have too little signal-to-noise (S/N) to measure reliable
flux density or polarization information. We combined over 5.2\,days of
archival data, at each of 1.5\,GHz and 2.0\,GHz, taken with the Green Bank
Telescope over the past 11\,years. We created high S/N profiles for 32 of the
pulsars and determined precise rotation measures (RMs) for 28 of them. We used
the RMs, and the known pulsar positions and dispersion measures (DMs), to map
the projected parallel component of the Galactic magnetic field toward the
cluster. The $\langle B_{||}\rangle$ shows a rough gradient of
$\sim$6\,nG/arcsec ($\sim$160\,nG/parsec), or fractionally, a change of
$\sim$20$\%$ in the right ascension direction across the cluster, implying
Galactic magnetic field variability at sub-parsec scales. We also measured
average flux densities $S_\nu$ for the pulsars, ranging from $\sim$10\,$\mu$Jy
to $\sim$2\,mJy, and an average spectral index $\alpha = -1.35$, where $S_\nu
\propto \nu^{\alpha})$. This spectral index is flatter than most known pulsars,
likely a selection effect due to the high frequencies used in pulsar searches
to mitigate dispersion and scattering. The inferred pulsar luminosity function
is roughly power-law, with slope $(d\log N)/(d\log L) = -1$ at the
high-luminosity end. At the low-luminosity end, there are incompleteness
effects implying that Terzan 5 contains many more pulsars to be found.
