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It is commonly believed that blazar jets are relativistic magnetized plasmaoutflows from supermassive black holes. One key question is how the jetsdissipate magnetic energy to accelerate particles and drive powerfulmulti-wavelength flares. Relativistic magnetic reconnection has been proposedas the primary plasma physical process in the blazar emission region. Recentnumerical simulations have shown strong acceleration of nonthermal particlesthat may lead to multi-wavelength flares. Nevertheless, previous works have notdirectly evaluated $\gamma$-ray signatures from first-principle simulations. Inthis paper, we employ combined particle-in-cell and polarized radiationtransfer simulations to study multi-wavelength radiation and opticalpolarization signatures under the leptonic scenario from relativistic magneticreconnection. We find harder-when-brighter trends in optical and {\itFermi-LAT} $\gamma$-ray bands as well as closely correlated optical and$\gamma$-ray flares. The optical polarization angle swings are also accompaniedby $\gamma$-ray flares with trivial time delays. Intriguingly, we find highlyvariable synchrotron self Compton signatures due to inhomogeneous particledistributions during plasmoid mergers. This feature may result in fast$\gamma$-ray flares or orphan $\gamma$-ray flares under the leptonic scenario,complementary to the frequently considered mini-jet scenario. It may also inferneutrino emission with low secondary synchrotron flux under the hadronicscenario, if plasmoid mergers can accelerate protons to very high energy.

Radiation and Polarization Signatures from Magnetic Reconnection in Relativistic Jets--II. Connection with $\gamma$-rays