  We derive NUV luminosity functions for 6471 NUV detected galaxies in 28 $0.02
< z < 0.08$ clusters and consider their dependence on cluster properties. We
consider optically red and blue galaxies and explore how their NUV LFs vary in
several cluster subsamples, selected to best show the influence of environment.
Our composite LF is well fit by the Schechter form with $M^*_{NUV}=-18.98 \pm
0.07$ and $\alpha=-1.87 \pm 0.03$ in good agreement with values for the Coma
centre and the Shapley supercluster, but with a steeper slope and brighter
$L^*$ than in Virgo. The steep slope is due to the contribution of massive
quiescent galaxies that are faint in the NUV. There are significant differences
in the NUV LFs for clusters having low and high X-ray luminosities and for
sparse and dense clusters, though none are particularly well fitted by the
Schechter form, making a physical interpretation of the parameters difficult.
When splitting clusters into two subsamples by X-ray luminosity, the ratio of
low to high NUV luminosity galaxies is higher in the high X-ray luminosity
subsample (i.e the luminosity function is steeper across the sampled luminosity
range). In subsamples split by surface density, when characterised by Schechter
functions the dense clusters have an $M^*$ about a magnitude fainter than that
of the sparse clusters and $\alpha$ is steeper ($-1.9$ vs. $-1.6$
respectively). The differences in the data appear to be driven by changes in
the LF of blue (star-forming) galaxies. This appears to be related to
interactions with the cluster gas [abridged]
