We have analysed the globular cluster (GC) system of the nucleated dwarf elliptical galaxy VCC 1087 in the Virgo cluster, based on Keck/LRIS spectroscopy and archival HST/ACS imaging. We estimate VCC 1087 hosts a total population of 77+/-19 GCs, which corresponds to a relatively high V-band specific frequency of 5.8+/-1.4. The g-z color distribution of the GCs shows a blue (metal-poor) peak with a tail of redder (metal-rich) clusters similar in color to those seen in luminous ellipticals. Spectroscopy of a subsample of 12 GCs suggests that the GC system is old and coeval (~10 Gyr), with a fairly broad metallicity distribution (-1.8<[m/H]<-0.8). In contrast, an integrated spectrum of the underlying galaxy starlight reveals that its optical luminosity is dominated by metal-rich, intermediate-aged stars. Radial velocities of the GCs suggest rotation close to the major axis of the galaxy, and this rotation is dynamically significant with (v/sigma)^* >1. A compilation of the kinematics of the GC systems of 9 early-type galaxies shows surprising diversity in the v/sigma parameter for GC systems. In this context, the GC system of VCC 1087 exhibits the most significant rotation to velocity dispersion signature. Modeling the velocity dispersion profile of the GCs and galaxy stars suggest fairly constant mass-to-light ratios of ~3 out to 6.5 kpc. The present observations can entertain both baryonic and non-baryonic solutions, and GC velocities at larger radii would be most valuable with regard to this issue. We discuss the evolution of VCC 1087 in terms of the galaxy ``harassment scenario, and conclude that this galaxy may well be the remains of a faded, tidally perturbed Sc spiral [abridged].
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