  Timing observations from the Parkes 64-m radio telescope for 165 pulsars
between 1990 and 2011 have been searched for period glitches. A total of 107
glitches were identified in 36 pulsars, where 61 have previously been reported
and 46 are new discoveries. Glitch parameters were measured by fitting the
timing residual data. Observed relative glitch sizes \Delta\nu_g/\nu range
between 10^-10 and 10^-5, where \nu = 1/P is the pulse frequency. We confirm
that the distribution of \Delta\nu_g/\nu is bimodal with peaks at approximately
10^-9 and 10^-6. Glitches are mostly observed in pulsars with characteristic
ages between 10^3 and 10^5 years, with large glitches mostly occurring in the
younger pulsars. Exponential post-glitch recoveries were observed for 27 large
glitches in 18 pulsars. The fraction Q of the glitch that recovers
exponentially also has a bimodal distribution. Large glitches generally have
low Q, typically a few per cent, but large Q values are observed in both large
and small glitches. Observed time constants for exponential recoveries ranged
between 10 and 300 days with some tendency for longer timescales in older
pulsars. Shorter timescale recoveries may exist but were not revealed by our
data which typically have observation intervals of 2 - 4 weeks. For most of the
36 pulsars with observed glitches, there is a persistent linear increase in
\dot\nu in the inter-glitch interval. Where an exponential recovery is also
observed, the effects of this are superimposed on the linear increase in
\dot\nu. In some cases, the slope of the linear recovery changes at the time of
a glitch. The \ddot\nu values characterising the linear changes in \dot\nu are
almost always positive and, after subtracting the magnetospheric component of
the braking, are approximately proportional to the ratio of |\dot\nu| and the
inter-glitch interval, as predicted by vortex-creep models.
