Fast Radio Burst 20180916B is a repeating FRB whose activity window has a 16.34 day periodicity that also shifts and varies in duration with the observing frequency. Recent observations report that the FRB has started to show an increasing trend in secular Rotation Measure (RM) after only showing stochastic variability around a constant value of -114.6rad/m^2^ since its discovery. RM studies let us directly probe the magnetic field structure in the local environment of the FRB. The trend of the variability can be used to constrain progenitor models of the FRB. Hence, further study of the RM variability forms the basis of this work. We studied the local environment of FRB 20180916B. We did so by focusing on polarization properties, namely RM, and studied how it varies with time. The data comes from the ongoing campaigns of FRB 20180916B using the upgraded Giant Metrewave Radio Telescope (uGMRT). The majority of the observations are in Band 4, which is centered at 650MHz with 200MHz bandwidth. Additionally, we used a few observations where we had simultaneous coverage in Band 4 and Band 5 (centered at 1100MHz). We apply a standard single pulse search pipeline to search for bursts. In total, we detect 116 bursts with ~36 hours of on-source time spanning 1200 days, with two bursts detected during simultaneous frequency coverage observations. We develop and apply a polarization calibration strategy suited for our dataset. On the calibrated bursts, we use QU-fitting to measure RM. Lastly, we also measure various other properties such as rate, linear polarization fraction and fluence distribution. Of the 116 detected bursts, we could calibrate 79 of them. From which, we observed in our early observations the RM continued to follow linear trend as modeled by arxiv:2205.09221. However, our later observations suggest the source switch from the linear trend to stochastic variations around a constant value of -58.75rad/m^2^. We also study cumulative rate against fluence and note that rate at higher fluences (>1.2Jy.ms) scales as {gamma}=-1.09(7) whereas that at lower fluences (between 0.2 and 1.2Jy.ms) only scales as {gamma}=-0.51(1), meaning rate at higher fluence regime is steeper than at lower fluence regime is steeper than at lower fluence regime. Lastly, we qualitatively assess the two extremely large bandwidth bursts that we detected in our simultaneous multi band observations. Future measurements of RM variations would help place stronger constraints on the local environment. Moreover, any periodic behavior in the RM measurements would directly test progenitor models. Therefore, we motivate such endeavors.