  We present the Atacama Large Millimeter/submillimeter Array (ALMA)
observations of linearly polarized 1.1 mm continuum emission at $\sim$0.14" (55
au) resolution and CO ($J$=2$-$1) emission at $\sim$1.5" (590 au) resolution
towards one prestellar (MMS 4), four Class 0 (MMS$\,$1, MMS$\,$3, MMS$\,$5, and
MMS$\,$6), one Class I (MMS$\,$7), and one flat-spectrum (MMS$\,$2) sources in
the Orion Molecular Cloud$\,$3 region. The dust disk-like structures and clear
CO outflows are detected towards all sources except for MMS$\,$4. The diameters
of these disk-like structures, ranging from 16 au to 97 au, are estimated based
on the deconvolved full width half maximum (FWHM) values obtained from the
multi-Gaussian fitting. Polarized emissions are detected towards MMS$\,$2,
MMS$\,$5, MMS$\,$6, and MMS$\,$7, while no polarized emission is detected
towards MMS$\,$1, MMS$\,$3, and MMS$\,$4. MMS$\,$2, MMS$\,$5, and MMS$\,$7 show
organized polarization vectors aligned with the minor axes of the disk-like
structures, with mean polarization fractions ranging from 0.6$\%$ to 1.2$\%$.
The strongest millimeter source, MMS$\,$6, exhibits complex polarization
orientations and a remarkably high polarization fraction of $\sim$10$\%$ around
the Stokes $I$ peak, and 15$-$20$\%$ on the arm-like structure, as reported by
Takahashi et al. (2019). The origins of the polarized emission, such as
self-scattering and dust alignment due to the magnetic field or radiative
torque, are discussed for individual sources. Some disk-like sources exhibit a
polarized intensity peak shift towards the nearside of the disk, which supports
that the polarized emission originates from self-scattering.
