  We investigate the relation of black hole mass versus host stellar mass and
that of mass accretion rate versus star formation rate (SFR) in moderately
luminous ($\log L_{\rm bol} \sim 44.5-46.5\ {\rm erg\ s^{-1}}$), X-ray selected
broad-line active galactic nuclei (AGNs) at $z=1.18-1.68$ in the
Subaru/XMM-Newton Deep Field. The far-infrared to far-ultraviolet spectral
energy distributions of 85 AGNs are reproduced with the latest version of Code
Investigating GALaxy Emission ({\tt CIGALE}), where the AGN clumpy torus model
{\tt SKIRTOR} is implemented. Most of their hosts are confirmed to be
main-sequence star-forming galaxies. We find that the mean ratio of the black
hole mass ($M_{\rm BH}$) to the total stellar mass ($M_{\rm stellar}$) is $\log
M_{\rm BH}/M_{\rm stellar} = -2.2$, which is similar to the local black
hole-to-bulge mass ratio. This suggests that if the host galaxies of these
moderately luminous AGNs at $z\sim1.4$ are dominated by bulges, they already
established the local black hole mass-bulge mass relation; if they are disk
dominant, their black holes are overmassive relative to the bulges. AGN
bolometric luminosities and SFR show a good correlation with ratios higher than
that expected from the local black hole-to-bulge mass relation, suggesting that
these AGNs are in a SMBH-growth dominant phase.
