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Both analytical and numerical works show that magnetic reconnection must occur in hot accretion flows.This process will effectively heat and accelerate electrons.In this paper we use the numerical hybrid simulation of magnetic reconnection plus test-electron method to investigate the electron acceleration and heating due to magnetic reconnection in hot accretion flows.We consider fiducial values of density, temperature, and magnetic parameter βe (defined as the ratio of the electron pressure to the magnetic pressure) of the accretion flow as n0～106cm-3, T0e～2×109K, and βe =1.We find that electrons are heated to a higher temperature Te=5×109K, and a fraction η～ 8％ of electrons are accelerated into a broken power-law distribution, dN(γ) ∝ γ-p, with p≈1.5 and 4 below and above ～1 MeV, respectively.We also investigate the effect of varying β and n0.We find that when βe is smaller or n0 is larger, i.e, the magnetic field is stronger, Te, η, and p all become larger.