  We report on a timing programme of 74 young pulsars that have been observed
by the Parkes 64-m radio telescope over the past decade. Using modern Bayesian
timing techniques, we have measured the properties of 124 glitches in 52 of
these pulsars, of which 74 are new. We demonstrate that the glitch sample is
complete to fractional increases in spin-frequency greater than
$\Delta\nu^{90\%}_{g}/\nu \approx 8.1 \times 10^{-9}$. We measure values of the
braking index, $n$, in 33 pulsars. In most of these pulsars, their rotational
evolution is dominated by episodes of spin-down with $n > 10$, punctuated by
step changes in the spin-down rate at the time of a large glitch. The step
changes are such that, averaged over the glitches, the long-term $n$ is small.
We find a near one-to-one relationship between the inter-glitch value of $n$
and the change in spin-down of the previous glitch divided by the inter-glitch
time interval. We discuss the results in the context of a range of physical
models.
