We present HST photometry of the late-type dwarf galaxy NGC 1705 observed with the WFPC2 in the F380W and F439W bands and with the ACS/HRC in the F330W , F555W , and F814W broad-band filters . We cross-correlate these data with previous ones acquired with the WFPC2 in the F555W , F814W bands , and derive multiband Color-Magnitude diagrams ( CMDs ) of the cross-identified individual stars and candidate star clusters . For the central regions of the galaxy , where HST-NICMOS F110W and F160W photometry is also available , we present U , B , V , I , J , H CMDs of the 256 objects with magnitudes measured in all bands . While our previous study based on F555W , F814W , F110W and F160W data allowed us to trace the star formation history of NGC 1705 back to a Hubble time , the new data provide a better insight on its recent evolution . With the method of the synthetic CMDs , we confirm the presence of two strong bursts of star formation ( SF ) . The older of the two bursts ( B1 ) occurred between \sim 10 and 15 Myr ago , coeval to the age of the central SSC . The younger burst ( B2 ) started \sim 3 Myr ago , and it is still active . The stellar mass produced by B2 amounts to \sim 10 ^ { 6 } M _ { \odot } , and it is a factor of \sim 3 lower for B1 . The interburst phase was likely characterized by a much lower level of star formation rather than by its complete cessation . The two bursts show distinct spatial distributions : while B1 is centrally concentrated , B2 is more diffused , and presents ring and arc-like structures that remind of an expanding shell . This suggests a feedback mechanism , in which the expanding superbubble observed in NGC 1705 , likely generated by the ( 10–15 ) Myr burst , triggered the current strong star formation activity . The excellent spatial resolution of the HRC allowed us to reliably identify 12 star clusters ( plus the SSC ) in the central \sim 26 " \times 29 " region of NGC 1705 , 10 of which have photometry in all the UBVIJH bands . The comparison of the cluster photometry with the GALEV populations synthesis models provides ages from \approx 10 Myr to \approx 1 Gyr , and masses between \approx 10 ^ { 4 } and 10 ^ { 5 } M _ { \odot } . The conspicuous cluster population in the central regions , with one super star cluster , one populous cluster and several regular ones , confirm the strong star forming activity of NGC 1705 .