[en] Recent studies of active galactic nuclei (AGNs) found a statistically inverse linear scaling between the X-ray normalized excess variance ${\mathrm{\sigma <!--\; ??\; -->}}_{\mathrm{r}\mathrm{m}\mathrm{s}}^2$ (variability amplitude) and the black hole (BH) mass spanning over $M_{\mathrm{B}\mathrm{H}}={10}^6-<!--\; ???\; -->{10}^9{M}_{\odot <!--\; ???\; -->}$. Suggested as having a small scatter, this scaling relation may provide a novel method to estimate the BH mass of AGNs. However, a question arises as to whether this relation can be extended to the low-mass regime below $\sim <!--\; ???\; -->{10}^6{M}_{\odot <!--\; ???\; -->}$. If confirmed, it would provide an efficient tool to search for AGNs with low-mass BHs using X-ray variability. This paper presents a study of the X-ray excess variances for a sample of AGNs with BH masses in the range of ${10}^5-<!--\; ???\; -->{10}^6{M}_{\odot <!--\; ???\; -->}$ observed with XMM-Newton and ROSAT, including data both from the archives and from newly preformed observations. It is found that the relation is no longer a simple extrapolation of the linear scaling; instead, the relation starts to flatten at $\sim <!--\; ???\; -->{10}^6{M}_{\odot <!--\; ???\; -->}$ toward lower masses. Our result is consistent with the recent finding of Ludlam et al. Such a flattening of the $M_{\mathrm{B}\mathrm{H}}-<!--\; ???\; -->{\mathrm{\sigma <!--\; ??\; -->}}_{\mathrm{r}\mathrm{m}\mathrm{s}}^2$ relation is actually expected from the shape of the power spectrum density of AGNs, for which the break frequency is inversely scaled with the mass of BHs.