  Using Monte Carlo simulations, we model the luminosity distribution of
recycled pulsars in globular clusters as the brighter, observable part of an
intrinsic distribution and find that the observed luminosities can be
reproduced using either log-normal or power-law distributions as the underlying
luminosity function. For both distributions, a wide range of model parameters
provide an acceptable match to the observed sample, with the log-normal
function providing statistically better agreement in general than the power-law
models. Moreover, the power-law models predict a parent population size that is
a factor of between two and ten times higher than for the log-normal models. We
note that the log-normal luminosity distribution found for the normal pulsar
population by Faucher-Gigu\`ere and Kaspi is consistent with the observed
luminosities of globular cluster pulsars. For Terzan~5, our simulations show
that the sample of detectable radio pulsars, and the diffuse radio flux
measurement, can be explained using the log-normal luminosity law with a parent
population of $\sim 150$ pulsars. Measurements of diffuse gamma-ray fluxes for
several clusters can be explained by both power-law and log-normal models, with
the log-normal distributions again providing a better match in general. In
contrast to previous studies, we do not find any strong evidence for a
correlation between the number of pulsars inferred in globular clusters and
globular cluster parameters including metallicity and stellar encounter rate.
