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Magakian et al. (2019) called attention to the current bright state of LkHa225 South, which over the past two decades has changed from $>20^m$ to $<13^m$.We present recent optical photometric monitoring that shows colorless,non-sinusoidal, periodic brightness variations. The oscillations occur every 43days, and have amplitude $\sim$0.7 mag with some variation among cycles. Wealso present new flux-calibrated optical and near-infrared spectroscopy, whichwe model in terms of a keplerian disk. Additional high dispersion spectrademonstrate the similarity of the absorption line pattern to some categories of"mixed temperature" accretion outburst objects. At blue wavelengths, LkHa 225South has a pure absorption spectrum and is a good spectral match to the FU Oristars V1515 Cyg and V1057 Cyg. At red optical and infrared wavelengths,however, the spectrum is more similar to Gaia 19ajj, showing emission in TiO,CO, and metals. Sr II lines indicate a low surface gravity atmosphere. Thereare also signatures of a strong wind/outflow. LkHa 225 South was moderatelybright in early 1950's as well as in late 1980's, with evidence for deep fadesduring intervening epochs. The body of evidence suggests that LkHa225 South isanother case of a source with episodically enhanced accretion that causesbrightening by orders of magnitude, and development of a hot absorptionspectrum and warm wind. It is similar to Gaia 19ajj, but also reminiscent inits long brightening time and brightness oscillation near peak, to the embeddedsources L1634 IRS7 and ESO Ha 99.

LkH$\alpha$ 225 (V1318 Cyg) South in Outburst