  Radio pulsar glitches probe far-from-equilibrium processes involving stress
accumulation and relaxation in neutron star interiors. Previous studies of
glitch rates have focused on individual pulsars with as many recorded glitches
as possible. In this work we analyze glitch rates using all available data
including objects that have glitched never or once. We assume the glitch rate
follows a homogeneous Poisson process, and therefore exclude pulsars which
exhibit quasiperiodic glitching behavior. Calculating relevant Bayes factors
shows that a model in which the glitch rate $\lambda$ scales as a power of the
characteristic age $\tau$ is preferred over models which depend arbitrarily on
powers of the spin frequency $\nu$ and/or its time derivative $\dot{\nu}$. For
$\lambda = A (\tau/\tau\vref)^{-\gamma}$, where $\tau_{\rm ref}=1\ {\rm yr}$ is
a reference time, the posterior distributions are unimodal with
$A=\ModelAAglitch\ \rm{yr}^{-1}$, and $\gamma=\ModelAgammaglitch$. Importantly,
the data exclude with 99\% confidence the possibility $\gamma=1$ canvassed in
the literature. When objects with zero recorded glitches are included, the
age-based rate law is still preferred and the posteriors change to give
$A=\ModelAAall\ \rm{yr}^{-1}$, and $\gamma=\ModelAgammaall$. The updated
estimates still support increased glitch activity for younger pulsars, while
demonstrating that the large number of objects with zero glitches contain
important statistical information about the rate, provided that they are part
of the same population as opposed to a disjoint population which never glitches
for some unknown physical reason.
