  We analyze the non--Gaussian primordial fluctuations which are inescapably
contributed by scalar fields $\Phi$ with vanishing expectation values,
$\langle\Phi\rangle=0$, present during inflation in addition to the inflaton
field. For simplicity we take $\Phi$ to be non--interacting and minimally
coupled to gravity. $\Phi$ is a Gaussian variable, but the energy density
fluctuations contributed by such a field are $\chi^2$--distributed. We compute
the three--point function $\xxxT$ for the configuration of an equilateral
triangle (with side length $\ell$) and the skewness $\dddRR$, {\it i.e.} the
third moment of the one--point probability distribution of the spatially
smeared energy density contrast $\de_R$, where $R$ is the smearing scale. The
relative magnitudes of the non--Gaussian effects,
$[\xi^{(N)}]^{1/N}/[\xi^{(2)}]^{1/2}$, do not grow in time. They are given by
numerical constants of order unity, independent of the scale $\ell$. The
"bi--skewness" $\dddRS$ is positive. For smearing lengths $R\ll S$ this shows
that in our model (in contrast to Gaussian models) voids are more quiet than
high--density regions.
