The rubble pile spin barrier is an upper limit on the rotation rate of asteroids larger than \sim 200 - 300 ~ { } m .
Among thousands of asteroids with diameters larger than \sim 300 ~ { } m , only a handful of asteroids are known to rotate faster than 2.0 ~ { } h , all are in the sub-km range ( \leq 0.6 ~ { } km ) .
Here we present photometric measurements suggesting that ( 60716 ) 2000 GD65 , an S-complex , inner-main belt asteroid with a relatively large diameter of 2.3 ^ { +0.6 } _ { -0.7 } ~ { } km , completes one rotation in 1.9529 \pm 0.0002 ~ { } h .
Its unique diameter and rotation period allow us to examine scenarios about asteroid internal structure and evolution : a rubble pile bound only by gravity ; a rubble-pile with strong cohesion ; a monolithic structure ; an asteroid experiencing mass shedding ; an asteroid experiencing YORP spin-up/down ; and an asteroid with a unique octahedron shape results with a four-peak lightcurve and a 3.9 ~ { } h period .
We find that the most likely scenario includes a lunar-like cohesion that can prevent ( 60716 ) 2000 GD65 from disrupting without requiring a monolithic structure or a unique shape .
Due to the uniqueness of ( 60716 ) 2000 GD65 , we suggest that most asteroids typically have smaller cohesion than that of lunar regolith .