  Understanding the interplay of stellar feedback and turbulence in the
interstellar medium (ISM) is essential to modeling the evolution of galaxies.
To determine the timescales over which stellar feedback drives turbulence in
the ISM, we performed a spatially resolved, multi-wavelength study of the
nearby star-forming dwarf galaxy UGC 4305 (aka Holmberg II). As indicators of
turbulence on local scales (400 pc), we utilized ionized gas velocity
dispersion derived from IFU H$\alpha$ observations and atomic gas velocity
dispersion and energy surface densities derived from HI synthesis observations
with the Very Large Array. These indicators of turbulence were tested against
star formation histories over the past 560 Myr derived from Color-Magnitude
Diagrams (CMD) using Spearman's rank correlation coefficient. The strongest
correlation identified at the 400 pc scale is between measures of HI turbulence
and star formation 70-140 Myr ago. We repeated our analysis of UGC 4305's
current turbulence and past star formation activity on multiple physical scales
($\sim$560, and 800 pc) to determine if there are indications of changes in the
correlation timescale with changes to the physical scale. No notable
correlations were found at larger physical scales emphasizing the importance of
analyzing star formation driven turbulence as a local phenomenon.
