  We present a high angular resolution ($\sim1"$) and wide-field ($2'.9 \times
1'.9$) image of the 1.3-mm continuum, CO($J$ = 2--1) line, and SiO($J$ = 5--4)
line emissions toward an embedded protocluster, FIR3, FIR4, and FIR5, in the
Orion Molecular Cloud 2 obtained from the Atacama Large
Millimeter/submillimeter Array (ALMA). We identify 51 continuum sources, 36 of
which are newly identified in this study. Their dust masses, projected sizes,
and $\mathrm{H_2}$ gas number densities are estimated to be $3.8 \times
10^{-5}$--$ 1.1 \times 10^{-2} \mathrm{M_{\odot}}$, 290--2000 au, and $6.4
\times 10^{6}$--$3.3 \times 10^{8}\,\mathrm{cm^{-3}}$, respectively. The
results of a Jeans analysis show that $\sim80\,\%$ of the protostellar sources
and $\sim15\,\%$ of the prestellar sources are gravitationally bound. We
identify 12 molecular outflows traced in the CO($J$ = 2--1) emission, six of
which are newly detected. We spatially resolve shocked gas structures traced by
the SiO($J$ = 5--4) emission in this region for the first time. We identify
shocked gas originating from outflows and other shocked regions. These results
provide direct evidence of an interaction between a dust condensation, FIR4,
and an energetic outflow driven by HOPS-370 located within FIR3. A comparison
of the outflow dynamical timescales, fragmentation timescales, and protostellar
ages shows that the previously proposed triggered star-formation scenario in
FIR4 is not strongly supported. We also discuss the spatial distribution of
filaments identified in our continuum image by comparing it with a previously
identified hub-fiber system in the $\mathrm{N_2H^+}$ line.
