  NGC 4395 is a dwarf Seyfert 1 galaxy with a possible intermediate-mass black
hole of several $\rm{10^4}$ solar masses in its center. As a well-studied
object, its broad line region size has been measured via H$\rm{\alpha}$ time
lag in numerous spectroscopic reverberation mapping (SRM) and narrow-band
photometric reverberation mapping (PRM) campaigns. Here we present its
H$\rm{\alpha}$ time lag measurement using broad-band photometric data, with the
application of our newly-developed ICCF-Cut method as well as the JAVELIN and
$\chi ^2$ methods. utilizing the minute-cadence multi-band light curves
obtained from the $\rm{2}$m FTN and $\rm{10.4}$m GTC telescopes in recent
works, we measured its H$\rm{\alpha}$ lag as approximately $40 \sim 90$ minutes
from broad-band PRM. With the H$\rm{\alpha}$ emission line velocity dispersion,
we calculated its central black hole mass as $\rm M_{\rm BH} = (8\pm4) \times
10^3\, M_{\rm \odot}$. These results are comparable with previous results
obtained by narrow-band PRM and SRM, providing further support to an
intermediate-mass black hole in NGC 4395. In addition, our study also validates
the ICCF-Cut as an effective method for broad-band PRM, which holds the
potential for widespread application in the era of large multi-epoch,
high-cadence photometric surveys.
