  We present near-infrared (observed frame) spectra of the high-redshift quasar
S4 0636+68 at z=3.2 which was previously thought to be one of a group of
``strong'' Fe II emitters [i.e., F(Fe II 4434-4684)/F(Hbeta) > 1]. Our K-band
spectrum clearly shows emission lines of Hbeta and [O III]4959, 5007 as well as
optical Fe II emission. Our computed value of F(Fe II 4434-4684)/F(Hbeta) ~ 0.8
for S4 0636+68 is less than previously thought, and in fact is comparable to
values found for radio-loud, flat-spectrum, low-z quasars. Therefore S4 0636+68
appears not to be a strong optical Fe II emitter. Although more than half (5/8)
of the high-z quasars observed to date are still classified as strong optical
Fe II emitters, their Fe II/Hbeta ratios, for the most part, follow the same
trend as that of low-$z$ quasars, i.e., an anticorrelation in EW(Fe
II)/EW(Hbeta) versus EW([O III])/EW(Hbeta), with radio-loud quasars having a
mean value of EW(Fe II)/EW(Hbeta) approximately half that of radio-quiet
quasars at comparable values of EW([O III])/EW(Hbeta).
