  Using the ALMA archival data of both CO(6--5) line and 689 GHz continuum
emission towards the archetypical Seyfert galaxy, NGC 1068, we identified a
distinct continuum peak separated by 14 pc from the nuclear radio component S1
in projection. The continuum flux gives a gas mass of ~2x10^5 Msun and
bolometric luminosity of ~10^8 Lsun, leading to a star formation rate of ~0.1
Msun/yr. Subsequent analysis on the line data suggest that the gas has a size
of ~10 pc, yielding to mean H2 number density of ~10^5 cm^{-3}. We therefore
refer to the gas as "massive dense gas cloud": the gas density is high enough
to form a "proto starcluster" whose stellar mass of ~10^4 Msun. We found that
the gas stands a unique position between galactic and extraglactic clouds in
the diagrams of start formation rate (SFR) vs. gas mass proposed by Lada et al.
and surface density of gas vs. SFR density by Krumholz and McKee. All the
gaseous and star-formation properties may be understood in terms of the
turbulence-regulated star formation scenario. Since there are two stellar
populations with the ages of 300 Myr and 30 Myr in the 100 pc-scale
circumnulear region, we discuss that NGC1068 has experienced at least three
episodic star formation events with a tendency that the inner star-forming
region is the younger. Together with several lines of evidence that the
dynamics of the nuclear region is decoupled from that of the entire galactic
disk, we discuss that the gas inflow towards the nuclear region of NGC 1068 may
be driven by a past minor merger.
