  The shape of the curves defined by the counts of radio sources per unit area
as a function of their flux density was one of the earliest cosmological
probes. Radio source counts continue to be an area of interest, used to study
the relative populations of galaxy types in the Universe (as well as
investigate any cosmological evolution in luminosity functions). They are a
vital consideration for determining how source confusion may limit the depth of
a radio interferometer observation, and are essential for characterising
extragalactic foregrounds in CMB experiments. There is currently no consensus
as to the relative populations of the faintest (sub-mJy) source types, where
the counts turn-up. Most of the source counts in this regime are gathered from
multiple observations that each use a deep, single pointing with a radio
interferometer. These independent measurements show large amounts of scatter
(factors ~ a few) that significantly exceeds their stated uncertainties. In
this article we use a simulation of the extragalactic radio continuum emission
to assess the level at which sample variance may be the cause of the scatter.
We find that the scatter induced by sample variance in the simulated counts
decreases towards lower flux density bins as the raw source counts increase.
The field-to-field variations are significant, and could even be the sole cause
at >100 {\mu}Jy. We present a method for evaluating the flux density limit that
a survey must reach in order to reduce the count uncertainty induced by sample
variance to a specific value. We also derive a method for correcting Poisson
errors on counts in order to include the uncertainties due to the cosmological
clustering of sources. An empirical constraint on the effect of sample variance
at these low luminosities is unlikely to arise until the completion of new
large-scale surveys with next-generation radio telescopes.
