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We present spectro-polarimetric analysis of \thisgrb\ using data from \asat,\fermi, and \swift, to provide insights into the physical mechanisms of theprompt radiation and the jet geometry.  Prompt emission from \thisgrb\ was very bright (fluence$>10^{-4}$~ergs~cm$^{-2}$) and had a complex structure composed of thesuperimposition of several pulses. The energy spectra deviate from the typicalBand function to show a low energy peak $\sim 15$~keV --- which we interpret asa power-law with two breaks, with a synchrotron origin. Alternately, the promptspectra can also be interpreted as Comptonized emission, or a blackbodycombined with a Band function. Time-resolved analysis confirms the presence ofthe low energy component, while the peak energy is found to be confined in therange of 100--200~keV.  Afterglow emission detected by \fermi-LAT is typical of an external shockmodel, and we constrain the initial Lorentz factor using the peak time of theemission. \swift-XRT measurements of the afterglow show an indication for a jetbreak, allowing us to constrain the jet opening angle to $>$ 6$\degr$.  Detection of a large number of Compton scattered events by \asat-CZTIprovides an opportunity to study hard X-ray polarization of the promptemission. We find that the burst has high, time-variable polarization, with theemission {\bf have higher polarization} at energies above the peak energy.  We discuss all observations in the context of GRB models and polarizationarising due to {\bf due to physical or geometric effects:} synchrotron emissionfrom multiple shocks with ordered or random magnetic fields, Poynting fluxdominated jet undergoing abrupt magnetic dissipation, sub-photosphericdissipation, a jet consisting of fragmented fireballs, and the Comptonizationmodel.

AstroSat-CZTI detection of variable prompt emission polarization in GRB 171010A