  This paper is the second in a series where we report the results of the
long-term timing of the millisecond pulsars (MSPs) in 47 Tucanae with the
Parkes 64-m radio telescope. We obtain improved timing parameters that provide
additional information for studies of the cluster dynamics: a) the pulsar
proper motions yield an estimate of the proper motion of the cluster as a whole
($\mu_{\alpha}\, = \, 5.00\, \pm \, 0.14\, \rm mas \, yr^{-1}$, $\mu_{\delta}\,
= \, -2.84\, \pm \, 0.12\, \rm mas \, yr^{-1}$) and the motion of the pulsars
relative to each other. b) We measure the second spin-period derivatives caused
by the change of the pulsar line-of-sight accelerations; 47 Tuc H, U and
possibly J are being affected by nearby objects. c) For ten binary systems we
now measure changes in the orbital period caused by their acceleration in the
gravitational field of the cluster. From all these measurements, we derive a
cluster distance no smaller than $\sim\,$4.69 kpc and show that the
characteristics of these MSPs are very similar to their counterparts in the
Galactic disk. We find no evidence in favour of an intermediate mass black hole
at the centre of the cluster. Finally, we describe the orbital behaviour of the
four "black widow" systems. Two of them, 47 Tuc J and O, exhibit orbital
variability similar to that observed in other such systems, while for 47 Tuc I
and R the orbits seem to be remarkably stable. It appears, therefore, that not
all "black widows" have unpredictable orbital behaviour.
