We derive two-dimensional dust attenuation maps at $sim1~mathrm{kpc}$ resolution from the UV continuum for ten galaxies on the $zsim2$ Star-Forming Main Sequence (SFMS). Comparison with IR data shows that 9 out of 10 galaxies do not require further obscuration in addition to the UV-based correction, though our sample does not include the most heavily obscured, massive galaxies. The individual rest-frame $V$-band dust attenuation (A$_{rm V}$) radial profiles scatter around an average profile that gently decreases from $sim1.8$ mag in the center down to $sim0.6$ mag at $sim3-4$ half-mass radii. We use these maps to correct UV- and H$alpha$-based star-formation rates (SFRs), which agree with each other. At masses $<10^{11}~M_{rm sun}$, the dust-corrected specific SFR (sSFR) profiles are on average radially constant at a mass-doubling timescale of $sim300~mathrm{Myr}$, pointing at a synchronous growth of bulge and disk components. At masses $>10^{11}~M_{rm sun}$, the sSFR profiles are typically centrally-suppressed by a factor of $sim10$ relative to the galaxy outskirts. With total central obscuration disfavored, this indicates that at least a fraction of massive $zsim2$ SFMS galaxies have started their inside-out star-formation quenching that will move them to the quenched sequence. In combination with other observations, galaxies above and below the ridge of the SFMS relation have respectively centrally-enhanced and centrally-suppressed sSFRs relative to their outskirts, supporting a picture where bulges are built due to gas `compaction that leads to a high central SFR as galaxies move towards the upper envelope of SFMS.
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