  With a mass of $\sim$1000 $M_\odot$ and a surface density of $\sim$0.5 g
cm$^{-2}$, G023.477+0.114 also known as IRDC 18310-4 is an infrared dark cloud
(IRDC) that has the potential to form high-mass stars and has been recognized
as a promising prestellar clump candidate. To characterize the early stages of
high-mass star formation, we have observed G023.477+0.114 as part of the ALMA
Survey of 70 $\mu$m Dark High-mass Clumps in Early Stages (ASHES). We have
conducted $\sim$1."2 resolution observations with the Atacama Large
Millimeter/submillimeter Array (ALMA) at 1.3 mm in dust continuum and molecular
line emission. We identified 11 cores, whose masses range from 1.1 $M_\odot$ to
19.0 $M_\odot$. Ignoring magnetic fields, the virial parameters of the cores
are below unity, implying that the cores are gravitationally bound. However,
when magnetic fields are included, the prestellar cores are close to virial
equilibrium, while the protostellar cores remain sub-virialized. Star formation
activity has already started in this clump. Four collimated outflows are
detected in CO and SiO. H$_2$CO and CH$_3$OH emission coincide with the
high-velocity components seen in the CO and SiO emission. The outflows are
randomly oriented for the natal filament and the magnetic field. The
position-velocity diagrams suggest that episodic mass ejection has already
begun even in this very early phase of protostellar formation. The masses of
the identified cores are comparable to the expected maximum stellar mass that
this IRDC could form (8-19 $M_\odot$). We explore two possibilities on how IRDC
G023.477+0.114 could eventually form high-mass stars in the context of
theoretical scenarios.
