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Our aim is to characterize the polarized continuum emission propertiesincluding intensity, polarization position angle, and polarization percentageof Sgr A* at $\sim$100 (3.0 mm), $\sim$230 (1.3 mm), $\sim$345 (0.87 mm),$\sim$500 (0.6 mm), and $\sim$700 GHz (0.43 mm). We report continuum emissionproperties of Sgr A* at the above frequency bands, based on the Atacama LargeMillimeter Array (ALMA) observations. We measured flux densities of Sgr A* fromALMA single pointing and mosaic observations. We performed sinusoidal fittingsto the observed (XX-YY)/I intensity ratios, to derive the polarization positionangles and polarization percentages. We successfully detect polarized continuumemission from all observed frequency bands. We observed lower Stokes Iintensity at $\sim$700 GHz than that at $\sim$500 GHz, which suggests thatemission at $\gtrsim$500 GHz is from optically thin part of a synchrotronemission spectrum. Both the Stokes I intensity and the polarization positionangle at our highest observing frequency of $\sim$700 GHz, may be varying withtime. However, we do not yet detect variation in the polarization percentage at$>$500 GHz. The polarization percentage at $\sim$700 GHz is likely lower thanthat at $\sim$500 GHz. By comparing the $\sim$500 GHz and $\sim$700 GHzobservations with the observations at lower frequency bands, we suggest thatthe intrinsic polarization position angle of Sgr A* is varying with time. Thispaper also reports the measurable polarization properties from the observedcalibration quasars. The future simultaneous multi-frequency polarizationobservations are required for clarifying the time and frequency variation ofpolarization position angle and polarization percentage.

Linearly Polarized Millimeter and Submillimeter Continuum Emission of Sgr A* Constrained by ALMA