  Approximately 8% of the $\sim$2800 known pulsars exhibit "nulling," a
temporary broadband cessation of normal pulsar emission. Nulling behaviour can
be coarsely quantified by the nulling fraction, which describes the percentage
of time a given pulsar will be found in a null state. In this paper, we perform
the most thorough statistical analysis thus far of the properties of 141 known
nulling pulsars. We find weak, non-linear correlations between nulling fraction
and pulse width, as well as nulling fraction and spin period which could be
attributed to selection effects. We also further investigate a
recently-hypothesized gap at 40% nulling fraction. While a local minimum does
exist in the distribution, we cannot confirm a consistent and unique break in
the distribution when we investigate with univariate and multivariate
clustering methods, nor can we prove the existence of two statistically
distinct populations about this minimum. Using the same methods, we find that
nulling pulsars are a statistically different population from normal, radio,
non-nulling pulsars, which has never been quantitatively verified. In addition,
we summarize the findings of the prior nulling pulsar statistics literature,
which are notoriously contradictory. This study, in context, furthers the idea
that nulling fraction alone does not contain enough information to describe the
behaviour of a nulling pulsar and that other parameters such as null lengths
and null randomness, in addition to a better understanding of selection
effects, are required to fully understand this phenomenon.
