  Glitches are rare spin-up events that punctuate the smooth slow-down of the
rotation of pulsars. For the Vela pulsar and PSR J0537-6910, the glitch sizes
and the times between consecutive events have clear preferred scales, contrary
to the handful of other pulsars with enough glitches for such a study.
Moreover, PSR J0537-6910 is the only pulsar showing a strong positive
correlation between the size of each glitch and the waiting time until the
following one.
  We attempt to understand this behavior through a detailed study of the
distributions and correlations of glitch properties for the eight pulsars with
at least ten detected glitches. We model the distributions of glitch sizes and
times between consecutive glitches for this sample and perform Monte Carlo
simulations to explore two hypotheses that could explain why the correlation is
so much weaker in other pulsars than in PSR J0537-6910.
  We confirm the above results for the Vela pulsar and PSR J0537-6910, and
verify that the latter is the only pulsar with a strong correlation between
glitch size and waiting time to the following glitch. For the remaining six
pulsars, the waiting time distributions are best fitted by exponentials, and
the size distributions either by power laws, exponentials, or log-normal
functions. Some pulsars in the sample yield significant Pearson and Spearman
coefficients ($r_p$ and $r_s$) for the aforementioned correlation. Moreover,
for all except the Crab, both coefficients are positive. Our simulations show
that the weaker correlations in pulsars other than PSR J0537$-$6910 cannot be
due to missing glitches too small to be detected. We also tested the hypothesis
that each pulsar may have two kinds of glitches, namely large, correlated ones
and small, uncorrelated ones. We found for all pulsars that their glitches are
not consistent with a pure uncorrelated population either.
