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We present a new ground-based visual transmission spectrum of the hot JupiterWASP-43b, obtained as part of the ACCESS Survey. The spectrum was derived fromfour transits observed between 2015 and 2018, with combined wavelength coveragebetween 5,300 \r{A}-9,000 \r{A} and an average photometric precision of 708 ppmin 230 \r{A} bins. We perform an atmospheric retrieval of our transmissionspectrum combined with literature HST/WFC3 observations to search for thepresence of clouds/hazes as well as Na, K, H$\alpha$, and $\rm H_2O$ planetaryabsorption and stellar spot contamination over a combined spectral range of5,318 \r{A}-16,420 \r{A}. We do not detect a statistically significant presenceof Na I or K I alkali lines, or H$\alpha$ in the atmosphere of WASP-43b. Wefind that the observed transmission spectrum can be best explained by acombination of heterogeneities on the photosphere of the host star and a clearplanetary atmosphere with $\rm H_2O$. This model yields a log-evidence of$8.26\pm0.42$ higher than a flat (featureless) spectrum. In particular, theobservations marginally favor the presence of large, low-contrast spots overthe four ACCESS transit epochs with an average covering fraction $f_\text{het}= 0.27^{+0.42}_{-0.16}$ and temperature contrast $\Delta T = 132\text{ K} \pm132\text{ K}$. Within the planet's atmosphere, we recover a log $\rm H_2O$volume mixing ratio of $-2.78^{+1.38}_{-1.47}$, which is consistent withprevious $\rm H_2O$ abundance determinations for this planet.

ACCESS: A Visual to Near-infrared Spectrum of the Hot Jupiter WASP-43b with Evidence of $\rm H_2O$, but no evidence of Na or K