  We present a study of the flux distribution of a sample of 15 Intermediate
and Low-energy peaked blazars using XMM-Newton observations in a total of 57
epochs on short-term timescales. We characterise the X-ray variability of all
of the light curves using excess fractional variability amplitude and found
that only 24 light curves in 7 sources are significantly variable. In order to
characterise the origin of X-ray variability in these blazars, we fit the flux
distributions of all these light curves using Gaussian and lognormal
distributions, as any non-Gaussian perturbation could indicate the imprints of
fluctuations in the accretion disc, which could be Doppler boosted through the
relativistic jets in blazars. However, intra-day variability, as seen in our
observations, is difficult to reconcile using disc components as the emissions
in such sources are mostly dominated by jets. We used Anderson-Darling (AD) and
$\chi^{2}$ tests to fit the histograms. In 11 observations of 4 blazars,
namely, ON 231, 3C 273, PKS 0235+164 and PKS 0521-365, both models equally fit
the flux distributions. In the rest of the observations, we are unable to model
them with any distribution. In two sources, namely, BL Lacertae and S4
0954+650, the lognormal distribution is preferred over the normal distribution,
which could arise from non-Gaussian perturbations from relativistic jets or
linear Gaussian perturbation in the particle time scale leading to such flux
distributions.
